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SWEEPS SWEEPS = Sagittarius Window Eclipsing Extrasolar Planet Search (Sahu et al. 2006) 7 day long stare of a field in the Galactic bulge, characterized by an old stellar population (about 10 billion years in age) 2 optical filters, V and I, and nearly continuous monitoring Sahu et al. found evidence for 16 extrasolar planets, with periods < 4.2 days follow-up epoch imaging of the same field 2 years later (Clarkson) to determine the space motions of stars 3

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Motivation: why study stellar flares? understand details of the flare process in vastly different stellar environments: does the solar model provide a good explanation of what we’re seeing? how do flares affect stellar environment, particularly in young stars or stars with planets? break through “foreground fog” of flare stars when searching for cosmological transient (interesting?) sources We have a very well-studied star at 1 AU, so why look any further? 4

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Stellar Flares The Sun flares, and cool stars with magnetic fields flare Flares occur as the result of the rearrangement of magnetic fields above the surface of a star They are seen as a sudden increase in intensity; and the entire atmosphere of a star participates in the flare Due to different physical processes at work, flares can be detected across the electro-magnetic spectrum (radio to gamma rays) Most flares are detected at optical and X-ray wavelengths 5

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What does a flare look like? 6 Credit: NASA Screenshot of an animation depicting the initiation of a solar flare. Download animation of this image (third from top in article) at http://www.nasa.gov/mission_pages/swift/bursts/monster_flare.html [Note: these are large files]

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How to Make a Flare I. Find a star whose interior has energy transfer by convection below the surface 7

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Find a young star (which is rotating rapidly because it is young), or alternatively, find a binary in which the two stars are tidally locked (orbital period = rotational period) How to Make a Flare II. 8

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Find a star which has evidence of spots on the surface, indicating magnetic fields emerging and interacting image of the Sun on July 28, 2011 How to Make a Flare III. 9

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the flare rate of stars declines with time, in concert with the decrease in the amount of magnetic fields the star can generate flaring at old age (several GY and beyond) can be seen from our Sun, and a few serendipitous measurements of stellar flares from single stars at ages of several billion years, tidally locked binaries can still produce flares the flare rate of old stars has not been systematically studied, due to the low expected flare rate 15

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Flares, Eclipses, & the SWEEPS dataset eclipsing extrasolar planets produce a DECREASE in the light from the star flares from the star INCREASE the star’s intensity SWEEPS data were taken in ~5 minute exposures, alternating the two filters the long timescale (1 week) and dense temporal coverage (cadence of ~10 minutes) of the dataset makes it ideal to search for flares in an older stellar population SWEEPS became DRAFTS (Deep, Rapid Archival Flare Transient Search), an archival HST project 16

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Finding Flares: we found flares on stars which show no underlying variations (top) and those which do (bottom) 17

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What we found Out of 229,701 stars that could be searched, 105 showed flares (128 flares total; some stars flared multiple times). The flare energies and peak intensities are consistent with those seen in nearby active stars (10 33 -10 35 ergs), and show a disconnect with solar flare behavior. Based on the star’s brightness, we saw modest flares in the brighter stars (flares increase of 10% or less in the star’s brightness) and larger flares in the fainter stars. A surprising fraction (85%) of flaring stars showed underlying variations, despite being a small component of the sample. This implies that the flaring rate is larger by a factor of 640 in the “variable” stars compared to the flat activity stars. 18

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Additionally, the stars exhibiting regular variations had a tendency to have short periods (less than 3 days) this is likely a signature of fast rotation, and the variations are caused by starspots the fast rotation could be a signpost of youth, or pointing towards an active binary 19

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What is the nature of the flaring stars? Their brightness and temperature are consistent with the old stellar population Their space motions look like the old stellar population They are likely not foreground young stars, but old binaries These binaries should have orbital periods equal to rotation periods, so can remain active for a long time These binaries must be much more common in the bulge than they are nearby approximate location of a solar-like star 20

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Impact on Planets the radiation of a flare can affect a planet’s atmosphere; only a small fraction of the high energy radiation can get to the planetary surface a significant flux of ultraviolet wavelength light may be able to damage the ozone layer of a planet, depending on the composition of the atmosphere most troublesome (and least quantifiable) is the ability of energetic particles to compress a planet’s magnetic field and expose the atmosphere to the radiation this research shows that flares are a force to be reckoned with in old stars 21

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Conclusions We have searched for flares in an old stellar population These flares are similar to those on active stars in the solar neighborhood The number of these active binaries in the bulge is larger than in the solar neighborhood, by a factor of > 20 Flares may pose a threat to planets around older stars, particularly planets around binaries (which we haven’t found yet) 22